Interstellar medium structure and the slope of the radio $\Sigma-D$ relation of supernova remnants

TL;DR

This study investigates how the fractal structure of the interstellar medium influences the radio surface brightness to diameter ($-D$) relation in supernova remnants, explaining steeper empirical slopes.

Contribution

It models the ISM as a fractal density structure and shows how this affects the $-D$ relation, providing insights into observed empirical slopes.

Findings

Fractal ISM structure can explain steeper observed $-D$ slopes.

Higher ambient density regions lead to steeper $-D$ slopes.

Geometrical effects and fractal structure influence the $-D$ relation, especially for older remnants.

Abstract

We analyze the influence of fractal structure of the interstellar matter (ISM) density on the parameter values for the radio surface brightness to diameter ($\Sigma-D$) relation for supernovae remnants (SNRs). We model a dense ISM as a molecular cloud with fractal density structure. SNRs are modelled as spheres of different radius scattered in the modelled ISM. The surface brightness of the SNRs is calculated from the simple relation $\Sigma \propto \rho^{0.5}D^{-3.5}$ and also from the parametrized more general form $\Sigma \propto \rho^{\eta}D^{-\beta_0}$. Our results demonstrate that empirical $\Sigma-D$ slopes that are steeper than the ones derived from theory, might be partly explained with the fractal structure of the ambient medium into which SNRs expand. The slope of the $\Sigma-D$ relation steepens if the density of the regions where SNRs are formed is higher. The simple geometrical effects combined with the fractal structure of the ISM can contribute to a steeper empirical $\Sigma-D$ slopes, especially for older remnants, and this is more pronounced if $\Sigma$ has a stronger dependence on ambient density.